J/ApJS/247/16 Extreme high-frequency-peaked BL Lac objects (Acciari+, 2020)
New hard-TeV extreme blazars detected with the MAGIC telescopes.
Acciari V.A., Ansoldi S., Antonelli L.A., Arbet Engels A., Asano K.,
Baack D., Babic A., Banerjee B., Barres de Almeida U., Barrio J.A.,
Becerra Gonzalez J., Bednarek W., Bellizzi L., Bernardini E., Berti A.,
Besenrieder J., Bhattacharyya W., Bigongiari C., Biland A., Blanch O.,
Bonnoli G., Bosnjak Z., Busetto G., Carosi R., Ceribella G., Cerruti M.,
Chai Y., Chilingaryan A., Cikota S., Colak S.M., Colin U., Colombo E.,
Contreras J.L., Cortina J., Covino S., D'Elia V., Da Vela P., Dazzi F.,
De Angelis A., De Lotto B., Delfino M., Delgado J., Depaoli D.,
Di Pierro F., Di Venere L., Do Souto Espineira E., Dominis Prester D.,
Donini A., Dorner D., Doro M., Elsaesser D., Fallah Ramazani V.,
Fattorini A., Ferrara G., Fidalgo D., Foffano L., Fonseca M.V., Font L.,
Fruck C., Fukami S., Garcia Lopez R.J., Garczarczyk M., Gasparyan S.,
Gaug M., Giglietto N., Giordano F., Godinovic N., Green D., Guberman D.,
Hadasch D., Hahn A., Herrera J., Hoang J., Hrupec D., Hutten M., Inada T.,
Inoue S., Ishio K., Iwamura Y., Jouvin L., Kerszberg D., Kubo H.,
Kushida J., Lamastra A., Lelas D., Leone F., Lindfors E., Lombardi S.,
Longo F., Lopez M., Lopez-Coto R., Lopez-Oramas A., Loporchio S.,
Machado de Oliveira Fraga B., Maggio C., Majumdar P., Makariev M.,
Mallamaci M., Maneva G., Manganaro M., Mannheim K., Maraschi L.,
Mariotti M., Martinez M., Mazin D., Micanovic S., Miceli D., Minev M.,
Miranda J.M., Mirzoyan R., Molina E., Moralejo A., Morcuende D., Moreno V.,
Moretti E., Munar-Adrover P., Neustroev V., Nigro C., Nilsson K., Ninci D.,
Nishijima K., Noda K., Nogues L., Nozaki S., Paiano S., Palatiello M.,
Paneque D., Paoletti R., Paredes J.M., Penil P., Peresano M., Persic M.,
Prada Moroni P.G., Prandini E., Puljak I., Rhode W., Ribo M., Rico J.,
Righi C., Rugliancich A., Saha L., Sahakyan N., Saito T., Sakurai S.,
Satalecka K., Schmidt K., Schweizer T., Sitarek J., Snidaric I.,
Sobczynska D., Somero A., Stamerra A., Strom D., Strzys M., Suda Y.,
Suric T., Takahashi M., Tavecchio F., Temnikov P., Terzic T., Teshima M.,
Torres-Alba N., Tosti L., Vagelli V., van Scherpenberg J., Vanzo G.,
Vazquez Acosta M., Vigorito C.F., Vitale V., Vovk I., Will M., Zaric D.,
Arcaro C., Carosi A., D'Ammando F., Tombesi F., Lohfink A.
<Astrophys. J. Suppl. Ser., 247, 16 (2020)>
=2020ApJS..247...16A 2020ApJS..247...16A
ADC_Keywords: BL Lac objects; Gamma rays; X-ray sources; Redshifts
Keywords: Blazars; Active galactic nuclei; Relativistic jets;
BL Lacertae objects; X-ray active galactic nuclei; Catalogs;
Non-thermal radiation sources; Gamma-ray sources
Abstract:
Extreme high-frequency-peaked BL Lac objects (EHBLs) are blazars that
exhibit extremely energetic synchrotron emission. They also feature
nonthermal gamma-ray emission whose peak lies in the very high-energy
(VHE, E>100GeV) range, and in some sources exceeds 1TeV: this is the
case for hard-TeV EHBLs such as 1ES 0229+200. With the aim of
increasing the EHBL population, 10 targets were observed with the
MAGIC telescopes from 2010 to 2017, for a total of 265hr of
good-quality data. The data were complemented by coordinated Swift
observations. The X-ray data analysis confirms that all but two
sources are EHBLs. The sources show only a modest variability and a
harder-when-brighter behavior, typical for this class of objects. At
VHE gamma-rays, three new sources were detected and a hint of a signal
was found for another new source. In each case, the intrinsic spectrum
is compatible with the hypothesis of a hard-TeV nature of these EHBLs.
The broadband spectral energy distributions (SEDs) of all sources are
built and modeled in the framework of a single-zone, purely leptonic
model. The VHE gamma-ray-detected sources were also interpreted with a
spine-layer model and a proton synchrotron model. The three models
provide a good description of the SEDs. However, the resulting
parameters differ substantially in the three scenarios, in particular
the magnetization parameter. This work presents the first mini catalog
of VHE gamma-ray and multiwavelength observations of EHBLs.
Description:
The final list of extreme high-frequency-peaked BL Lac (EHBLs) targets
observed with the MAGIC telescopes located on the Canary island of La
Palma is summarized in Table 1.
Ten targets were observed with the MAGIC telescopes from 2010-2017. A
total of 265hr of good-quality data were collected and analyzed.
Table 2 summarizes the general information of MAGIC observations.
For the determination of the high energy gamma-ray properties of the
sources of this study, the analysis of Fermi-LAT data was performed.
The details of the analysis are reported in Table 4 (see appendix B
and Section 4).
When possible, Swift-XRT data simultaneous with MAGIC pointings were
requested via Target of Opportunity (ToO) observations. Moreover, all
of the available Swift-XRT archival data have been analyzed using the
procedure detailed in Appendix C.
NuSTAR observed TXS 0210+515 and RGB J2313+147 in the hard X-ray band
(3-79keV) with its two coaligned X-ray telescopes with corresponding
focal planes, focal plane module A (FPMA) and B (FPMB), on 2016
January 30 and 2015 May 30, for a net exposure time of 21.4ks and
22.9ks, respectively.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 77 11 Sample of extreme high-frequency-peaked BL Lac
targets (EHBLs) observed with the MAGIC telescopes
table2.dat 69 13 Results of the signal search and integral flux
analysis of the MAGIC data for the 10 EHBLs
considered in this study
table4.dat 82 11 Main spectral parameters resulting from the
analysis of Swift-XRT and Fermi-LAT data
table6.dat 59 11 Main spectral parameters from the 3FGL, 2FHL, and
3FHL catalogs
table7.dat 117 319 The Swift-XRT results for the 11 sources
table8.dat 79 11 Main spectral parameters resulting from combining
all Swift-XRT pointings during the MAGIC
observation window
fig1.dat 109 36 Spectral energy distributions (Data behind Figure 1)
fig3.dat 124 166 Broadband SED and modeled spectra
(Data behind Figure 3)
fig4.dat 105 101 Broadband SED and modeled spectra for the four
sources with no MAGIC detection or hints (but
Fermi-LAT detection); i.e. 1ES 0927+500,
BZB J0809+3455, RGB J2313+147 and TXS 0637-128
(Data behind Figure 4)
fig10.dat 105 19 SED of RBS 0921 (Data behind Figure 10)
--------------------------------------------------------------------------------
See also:
B/swift : Swift Master Catalog (HEASARC, 2004-)
VIII/76 : Leiden/Argentine/Bonn (LAB) Survey of Galactic HI (Kalberla+ 2005)
V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012)
J/A+A/379/755 : Radio data of X- & gamma-ray blazars (Venturi+, 2001)
J/A+A/436/799 : X- & gamma-ray fluxes of blazars (Fan, 2005)
J/ApJ/626/95 : Gamma-ray blazar candidates (Sowards-Emmerd+, 2005)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/709/1407 : SED of the Fermi blazars (Li+, 2010)
J/ApJ/716/30 : SED of Fermi bright blazars (Abdo+, 2010)
J/other/NewA/16.503 : 2MASS observation of BL Lac objects II. (Mao+, 2011)
J/ApJ/761/125 : X & γ spectral indexes of blazars (Fan+, 2012)
J/A+A/541/A160 : Planck + X/γ obs. of blazars (Giommi+, 2012)
J/ApJS/207/16 : BL Lac candidates for TeV observations (Massaro+, 2013)
J/ApJS/209/34 : The first Fermi-LAT >10GeV cat. (1FHL) (Ackermann+, 2013)
J/ApJ/764/135 : Spectroscopic redshifts of BL Lac objects (Shaw+, 2013)
J/ApJ/789/135 : Gamma-ray bright blazars spectrophot. (Williamson+, 2014)
J/ApJS/218/23 : Fermi LAT third source catalog (3FGL) (Acero+, 2015)
J/ApJS/222/5 : 2nd Fermi-LAT >50GeV catalog (2FHL) (Ackermann+, 2016)
J/MNRAS/458/56 : TeV gamma-ray blazar X-ray studies (Wierzcholska+, 2016)
J/AJ/151/142 : Five yrs of blazar obs. with VERITAS (Archambault+, 2016)
J/ApJS/224/26 : SEDs of Roma BZCAT blazars (Mao+, 2016)
J/ApJS/226/20 : X-ray, opt. & radio SEDs of Fermi blazars (Fan+, 2016)
J/ApJS/232/18 : The third Fermi-LAT >10GeV catalog (3FHL) (Ajello+, 2017)
J/ApJS/233/17 : Swift/BAT AGN spectrosc. survey. V. X-ray (Ricci+, 2017)
J/A+A/598/A17 : The 2WHSP catalog (Chang+, 2017)
J/A+A/608/A68 : TeV/non-TeV BL Lacs fluxes (Fallah Ramazani+, 2017)
J/ApJ/864/84 : Swift follow-up obs. of TXS 0506+056 (Keivani+, 2018)
J/ApJS/235/4 : 105-month Swift-BAT all-sky hard X-ray survey (Oh+, 2018)
J/A+A/631/A150 : Softly X-raying the gamma-ray sky I. (Marchesini+, 2019)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Target name
16 A1 --- f_Name [f] f: reference source (1)
18- 23 F6.2 deg RAdeg Right ascension in decimal degrees (J2000)
25- 30 F6.2 deg DEdeg Declination in decimal degrees (J2000)
32- 37 F6.2 deg GLON [67.7/249.3] Galactic longitude
39- 44 F6.2 deg GLAT [-42/65] Galactic latitude
46- 50 F5.3 --- z [0.049/0.3] Redshift
52 A1 --- r_z [a-e] Redshift reference (2)
54- 58 F5.3 10+21cm-2 NH [0.1/4.4] Equivalent galactic hydrogen
column density reported by
Kalberla+ (2005, VIII/76)
60- 63 F4.1 Hz lognuPk [16.6/18.5]? Synchrotron peak frequency
reported by Chang+ (2017, J/A+A/598/A17)
65- 77 A13 --- Sel Selection criteria (3)
--------------------------------------------------------------------------------
Note (1):
f = The sample includes the archetypal Extreme high-frequency-peaked BL Lac
(EHBL) source 1ES 0229+200, which has been deeply observed by MAGIC
between 2013 and 2017 and is added as a reference source (MAGIC
Collaboration et al. 2019MNRAS.486.4233A 2019MNRAS.486.4233A & MAGIC Collaboration 2019,
in preparation).
Note (2): Reference as follows:
a = Mao (2011, J/other/NewA/16.503).
b = S. Paiano (2020, in preparation).
c = Ahn et al. (2012, V/139).
d = Shaw et al. (2013, J/ApJ/764/135).
e = Sowards-Emmerd et al. (2005, J/ApJ/626/95).
Note (3): Criteria adopted for the selection as follows:
i = hard spectral index (Γ≤2) in the soft X-ray band covered
by Swift-XRT
ii = High energy (HE) gamma-ray emission extracted from the following LAT
catalogs: the 1FHL, the First Fermi-LAT Catalog of Sources above
10GeV (Ackermann+ 2013, J/ApJS/209/34), the 2FHL (Ackermann+
2016, J/ApJS/222/5), and the 3FGL, the Fermi-LAT 4yr Point Source
Catalog (Acero+ 2015, J/ApJS/218/23).
iii = in the list of EHBL candidates proposed in
Bonnoli+ (2015MNRAS.451..611B 2015MNRAS.451..611B), where the authors propose new
candidates according to the high X-ray-to-radio flux ratio
iv = best candidates from Fallah Ramazani+ (2017, J/A+A/608/A68) whose
X-rays and HE gamma-ray properties follow criteria (i) and (ii).
v = low-redshift (<0.2) sources.
See Section 2 for further details.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Target name
16- 31 A16 yr Date Year(s) of observation
33- 37 F5.1 h Exp [5.9/117.5] Effective exposure time
after quality cuts
39- 42 F4.1 --- Sigma [-0.9/9] Significance of the signal
in σ
44- 46 I3 GeV Eth [150/300] Assumed energy threshold for
integral flux calculation
48- 48 A1 --- l_Flux Limit flag on Flux (4)
49- 51 F3.1 10-12cm-2/s Flux [1.5/9.3] Flux measured above the energy
threshold
53- 55 F3.1 10-12cm-2/s e_Flux [0.3/1.1]? Flux uncertainty
57 A1 --- f_Flux [gh] Flag on Flux (5)
59- 59 A1 --- l_Lum Limit flag on Lum (4)
60- 63 F4.1 10+36W Lum [0.6/68.5] VHE gamma-ray luminosity
over 200GeV; in 1043erg/s units
65- 67 F3.1 10+36W e_Lum [0.2/4.8]? Lum uncertainty
69 A1 --- VHE? [YNH] Source detection status at very
high-energy (E>100GeV) gamma-rays (6)
-------------------------------------------------------------------------------
Note (4): In case of nondetection (see Section 3 for details), an integral flux
upper limit is reported instead, assuming a simple power-law spectrum
of spectral index Γ (see Equation (1) and the text for further
details).
Note (5): Flag as follows:
g = Flux upper limit is calculated by assuming the observed photon index
Γobs=2.0.
h = Flux upper limit is calculated by assuming the observed photon index
Γobs=2.6 derived from 2012 observations.
Note (6): Status as follows:
Y = detected,
N = not detected,
H = hint of signal.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Target name
16 A1 --- n_Name [b] Note on name (1)
18- 22 I5 d MJDx [55648/57784] Swift-XRT observation date
24- 27 F4.1 10-15W/m2 F2-10keV [1.6/47.4] Swift-XRT X-ray flux in
the 2-10keV energy range
29- 31 F3.1 10-15W/m2 e_F2-10keV [0.1/1.4] Fxrt uncertainty
33- 36 F4.2 --- GammaX [1.63/2.18] Spectral index of
X-ray spectrum
38- 41 F4.2 --- e_GammaX [0.02/0.2] GammaX uncertainty
43- 47 F5.1 --- chi2 [9.5/171.2] Fit χ2
48 A1 --- --- [/]
49- 51 I3 --- dof [14/172] Degree of freedom
53- 57 I5 d MJDSt [54682/57388]? Fermi-LAT start date
of observation
58 A1 --- --- [-]
59- 63 I5 d MJDEnd [56292/58318]? Fermi-LAT end date
of observation
65- 67 F3.1 10-10cm-2/s F1-300GeV [1.4/6.7]? Fermi-LAT gamma-ray flux
in the range of 1-300GeV
69- 71 F3.1 10-10cm-2/s e_F1-300GeV [0.6/1.7]? Ffermi uncertainty
73- 75 F3.1 --- GammaR [1.4/2]? Spectral index of
the HE gamma-ray spectrum
77- 79 F3.1 --- e_GammaR [0.2/0.2]? GammaR uncertainty
81- 82 I2 --- TS [23/94] Likelihood test statistics (TS)
of the fitted model (2)
--------------------------------------------------------------------------------
Note (1):
b = The X-ray energy range for spectral analysis is 1.5-10keV
(see Appendix C for details).
Note (2): The square root of the TS is approximately equal to the detection
significance for a given source.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Target name
16- 19 F4.2 10-10ph/cm2/s F1-100GeV [1.8/6.6]? 3FGL gamma-ray flux
in 1-100 GeV energy range
21- 24 F4.2 10-10ph/cm2/s e_F1-100GeV [0.1/1]? F3FGL uncertainty
26- 29 F4.2 --- Gam3FGL [1.4/2.1]? Spectral index for the
power-law fit in 100MeV-100GeV
31- 34 F4.2 --- e_Gam3FGL [0.08/0.3]? Gam3FGL uncertainty
36- 39 F4.1 --- Sig [5.1/16.7]? the detection significance
reported by 3FGL
(Acero+ 2015, J/ApJS/218/23)
41- 44 F4.2 --- Gam3FHL [1.5/2.1]? Spectral index for the
power-law fit >10GeV reported in 3FHL
(Ajello+ 2017, J/ApJS/232/18)
46- 49 F4.2 --- e_Gam3FHL [0.1/0.4]? Gam3FHL uncertainty
51- 54 F4.2 --- Gam2FHL [1.09/3.6]? Spectral index for the
power-law fit >50GeV reported in 2FHL
(Ackermann+ 2016, J/ApJS/222/5)
56- 59 F4.2 --- e_Gam2FHL [0.4/1.4]? Gam2FHL uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Source identifier
16- 23 F8.2 d MJD Modified Julian Date of observation
25- 35 I11 --- obsid Observation identifier
37- 40 I4 s Exp [48/6905] Exposure time
42- 45 F4.2 --- GammaPL [1.3/2.4]? Spectral index of power
law-model (1)
47- 50 F4.2 --- e_GammaPL [0.02/0.3]? Uncertainty in GammaPL
52- 56 F5.1 --- chi2PL [0.3/172]? Power law-model χ2
58- 60 I3 --- dofPL [2/172]? Power law-model Degrees of Freedom
62- 65 F4.2 --- GammaLP [1.3/2.1]? Spectral index of log-parabola
model (1)
67- 70 F4.2 --- e_GammaLP [0.05/0.2]? Uncertainty in GammaLP
72- 75 F4.2 --- betaLP [0.2/1]? Curvature parameter of fitted
log-parabola model
77- 80 F4.2 --- e_betaLP [0.09/0.3]? Uncertainty in betaLP
82- 86 F5.1 --- chi2LP [7.5/109]? log-parabola model χ2
88- 90 I3 --- dofLP [18/114]? log-parabola model Degrees
of Freedom
92- 96 F5.2 % Prob Null-hypotheses of probability of F-test (2)
98-101 F4.1 10-15W/m2 F2-10 [1.5/85] X-ray 2-10 keV flux density (3)
103-106 F4.1 10-15W/m2 e_F2-10 [0.1/14] Uncertainty in F2-10 (3)
108-112 F5.1 10-15W/m2 F0.3-10 [2.8/140] X-ray 0.3-10 keV flux density (3)
114-117 F4.1 10-15W/m2 e_F0.3-10 [0.1/13] Uncertainty in F0.3-10 (3)
--------------------------------------------------------------------------------
Note (1): The range for spectral analysis is 0.3-10keV except for the source
1ES 2037+521 for which the spectral analysis range is between
1.5 and 10keV.
Note (2): The log-parabola model is preferred over power-law model with 3 sigma
confidence level if the F-test probability value is ≤0.27%.
Note (3): In units of 1e-12erg/s/cm2.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Target name
16 A1 --- n_Name [c] Note on Name (7)
18- 22 I5 d MJDSt [55641/57775] Start date of observation
23 A1 --- --- [-]
24- 28 I5 d MJDEnd [55649/58055] End date of observation
30- 34 F5.2 10-15W/m2 F2-10keV [1.5/45.5] Swift-XRT 2-10keV X-ray flux
during MAGIC observation window
36- 39 F4.2 10-15W/m2 e_F2-10keV [0.03/1.2] F2-10keV uncertainty
41- 44 F4.2 --- Gamma [1.4/2.2] Spectral index
46- 49 F4.2 --- e_Gamma [0.02/0.2] Gamma uncertainty
51- 54 F4.2 --- beta [0.2/0.6]? Curvature parameter of
the log-parabola model
56- 59 F4.2 --- e_beta [0.04/0.2]? beta uncertainty
61- 65 F5.1 --- chi2 [30.5/398] χ2 fit
66 A1 --- --- [/]
67- 69 I3 --- dof [32/377] Degree of freedom
71- 74 F4.2 --- GamEq [1.9/2.4]? Equivalent spectral index when
the log parabola is the best-fit model
76- 79 F4.2 --- e_GamEq [0.05/0.3]? GamEq uncertainty
--------------------------------------------------------------------------------
Note (7):
c = The range for spectral analysis is 1.5-10keV (see text for details).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- Name Source identifier
15- 22 F8.3 GeV Energy [144.7/3774] Energy
24- 32 F9.4 GeV e_Energy [31.5/1210]? Lower Energy bin width
34- 42 F9.4 GeV E_Energy [41/2489]? Upper Energy bin width
44- 54 E11.5 1/TeV/cm2/s dN/dE [2.4e-14/7.5e-11] Differential photon flux
at Energy
56- 66 E11.5 1/TeV/cm2/s e_dN/dE Lower uncertainty in dN/dE
68- 78 E11.5 1/TeV/cm2/s E_dN/dE Upper uncertainty in dN/dE
80- 84 I5 d Start [56035/57658] Modified Julian start date
of observation
86- 90 I5 d End [56066/58056] Modified Julian end date
of observation
92- 95 F4.1 h Texp [8.7/52.5] Exposure time
97-109 A13 --- Comm Comment (1)
--------------------------------------------------------------------------------
Note (1): Comment as follows:
observed = Observed data point.
EBL corrected = Extragalactic background light corrected data point.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: fig[34].dat fig10.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- Name Source identifier
16- 23 E8.2 Hz Freq [4.86e+14/9.13e+26] Frequency
25- 32 E8.2 Hz e_Freq ? Lower 1σ uncertainty limit in Freq
34- 41 E8.2 Hz E_Freq ? Upper 1σ uncertainty limit in Freq
43 A1 --- l_nufnu Upper limit flag on nufnu
44- 51 E8.2 mW/m2 nufnu [3.14e-13/2.66e-11] Differential photon flux
at Freq; in units of erg/s/cm2
53- 60 E8.2 mW/m2 e_nufnu ? Lower 1σ uncertainty limit in nufnu
62- 69 E8.2 mW/m2 E_nufnu ? Upper 1σ uncertainty limit in nufnu
71- 78 F8.2 d Start [54682/57784]? Modified Julian start date
of observation
80- 87 F8.2 d End [55648/58319]? Modified Julian end date
of observation
89- 94 I6 s Texp [1506/423000]? Exposure time
96-124 A29 --- Comm Comment(s)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 27-Apr-2020